  [Abridge] In the first paper of this series (paper I) we presented a new
approach for studying the chemo-odynamical evolution in disk galaxies, focusing
on the Milky Way. Here we extend these results to different distances from the
Galactic center, looking for variations of observables that can be related to
on-going and future spectroscopic surveys. By separating the effects of
kinematic heating and radial migration, we show that migration is much more
important, even for the oldest and hottest stellar population. The
distributions of stellar birth guiding radii and final guiding radii
(signifying contamination from migration and heating, respectively) widen with
increasing distance from the Galactic center. As a result, the slope in the
age-metallicity relation flattens significantly at Galactic radii larger than
solar. The radial metallicity and [Mg/Fe] gradients in our model show
significant variations with height above the plane due to changes in the
mixture of stellar ages. An inversion in the radial metallicity gradient is
found from negative to weakly positive (at r<10 kpc), and from positive to
negative for the [Mg/Fe] gradient, with increasing distance from the disk
plane. We relate this to the combined effect of (i) the predominance of young
stars close to the disk plane and old stars away from it, (ii) the more
concentrated older stellar component, and (iii) the flaring of mono-age disk
populations. We also investigate the effect of recycled gas flows on the mean
[Fe/H] and find that in the region 4<r<12 kpc the introduced errors are less
than 0.05-0.1 dex, related to the fact that inward and outward flows mostly
cancel in that radial range. We show that radial migration cannot compete with
the inside-out formation of the disk, exposed by the more centrally
concentrated older disk populations, and consistent with recent observations.
