Abstract: The derivation of precise stellar ages is considered the current major challenge to reconstruct the chronology of the Milky Way. We have shown that CMD-fitting offers a robust alternative to individual age determinations via the derivation of global (dynamically evolved) star formation histories (SFH) and age-metallicity distributions (Gallart et al. 2024). As part of the ChronoGal project we are computing stellar age-metallicity distributions for vast samples of stars within the extended Solar neighbourhood (up to 1-3.5 Kpc from the Sun, depending on the direction). Improving upon our previous works (Gallart et al. 2019, Ruiz-Lara et al 2020), in this talk we present our updated set of routines ('CMDft.Gaia') to obtain SFHs from Gaia CMDs, with which we have obtained the most precise characterisation -in terms of ages- of the stellar populations in the solar neighbourhood. We are now studying, using Gaia DR3, the first spatially-resolved SFHs across the Milky Way disks, and kinematically selected thin and thick disc and halo stars. They show that distinct star formation episodes contribute differently as a function of height from the plane and galactocentric radius, thus providing clear insights about the formation process of our Galactic disk. Kinematically selected populations in the same volume have distinct SFH with, in the case of the halo, signatures that can be identified with Gaia-Enceladus and the splashed disk. These results allow us to provide strong new insights into long lasting question in Galactic Archaeology that require information on the age dimension.