Detailed studies of the stellar populations of intermediate-redshift galaxies can shed light onto the processes responsible for the growth of the massive galaxy population in the last 8 billion years. We measure velocity dispersion and stellar absorption features for individual sources. We interpret them by means of a large Monte Carlo library of star formation histories, following the Bayesian approach adopted for previous low redshift studies, and derive constraints on the stellar mass, mean stellar age, and stellar metallicity of these galaxies. We characterize for the first time the relations between stellar age and stellar mass and between stellar metallicity and stellar mass at z ~ 0.7 for the galaxy population as a whole and for quiescent and star-forming galaxies separately. However, other observations require the quiescent population to grow from z = 0.7 to the present day. This indicates chemical enrichment until the present in at least a fraction of the z = 0.7 star-forming galaxies in our sample.