The kinematic properties of the stellar subpopulations in the Milky Way disc are linked to their radial and vertical scale lengths. On the other hand, element abundances and abundance ratios are a signature of the evolution history of the stellar components. Large spectroscopic surveys like SEGUE, RAVE, APOGEE and Gaia-ESO, combined with proper motions and distances (ultimately from the Gaia mission starting with the TEGAS data release in Sept. 2016) are linking the kinematic and chemical properties and provide powerful tests of any Milky Way model. Our self-consistent local disc model (the JJ-model) with the star formation history (SFR), the dynamical evolution (AVR) and stellar evolution as ingredients reproduces the local kinematics of main sequence stars, SDSS star counts towards the North Galactic Pole, and the metallicity distribution of G dwarfs very well. From local star counts the IMF is determined and we derive the age-metallicity relation (AMR) and the gas infall rate using the alpha-element and iron distributions. Radially extended data from APOGEE and other surveys allow an insight in the inside-out growth of the Milky Way thin disc. Correlations of radial gradients in density, kinematics, abundances, and age are crucial to constrain the evolution scenario of the Milky Way disc.