Aims. The high abundances of CH+ in the diffuse interstellar medium (ISM) are a long-standing issue of our understanding of the thermodynamical and chemical states of the gas. We investigate here the formation of CH + in turbulent and multiphase environments, where the heating of the gas is almost solely driven by the photoelectric effect. Methods. The diffuse ISM is simulated using the magnetohydrodynamic (MHD) code RAMSES which self-consistently computes the dynamical and thermal evolution of the gas along with the time-dependent evolutions of the abundances of H + , H, and H 2 . The rest of the chemistry, including the abundance of CH + , is computed in post-processing, at equilibrium, under the constraint of out-of-equilibrium H + , H, and H 2 . The comparison with the observations is performed taking into account an often neglected yet paramount piece of information, namely the length of the intercepted diffuse matter along the observed lines of sight. Results. Almost all of the mass of CH + originates from unstable gas, in environments where the kinetic temperature is higher than 600 K, the density ranges between 0.6 and 10 cm −3 , the electronic fraction ranges between 3 × 10 −4 and 6 × 10 −3 , and the molecular fraction is smaller than 0.4. Its formation is driven by warm and out-of-equilibrium H 2 initially formed in the cold neutral medium (CNM) and injected in more diffuse environments, and even the warm neutral medium (WNM) through a combination of advection and thermal instability. The simulation that displays the closest agreement with the HI-to-H 2 transition and the thermal pressure distribution observed in the solar neighborhood is found to naturally reproduce the observed abundances of CH + , the dispersion of observations, the probability of occurrence of most of the lines of sight, the fraction of nondetections of CH + , and the distribution of its line profiles. The amount of CH + and the statistical properties of the simulated lines of sight are set by the fraction of unstable gas rich in H 2 , which is controlled on Galactic scales by the mean density of the diffuse ISM (or, equivalently, its total mass), the amplitude of the mean UV radiation field, and the strength of the turbulent forcing. Conclusions. This work offers a new and natural solution to an 80-yr-old chemical riddle. The almost ubiquitous presence of CH + in the diffuse ISM likely results from the exchange of matter between the CNM and the WNM induced by the combination of turbulent advection and thermal instability, without the need to invoke ambipolar diffusion or regions of intermittent turbulent dissipation. Through two-phase turbulent mixing, CH + might thus be a tracer of the H 2 mass loss rate of CNM clouds.