  We present dynamical scaling relations, combined with the stellar population
properties, for a subsample of about 6000 nearby galaxies with the most
reliable dynamical models extracted from the full MaNGA sample of 10K galaxies.
We show that the inclination-corrected mass plane (MP) for both early-type
galaxies (ETGs) and late-type galaxies (LTGs), which links dynamical mass,
projected half-light radius $R_{\rm e}$, and the second stellar velocity moment
$\sigma_{\rm e}$ within $R_{\rm e}$, satisfies the virial theorem and is even
tighter than the uncorrected one. We find a clear parabolic relation between
$\lg(M/L)_{\rm e}$, the total mass-to-light ratio within a sphere of radius
$R_{\rm e}$, and $\lg\sigma_{\rm e}$, with the $M/L$ increasing with
$\sigma_{\rm e}$ and for older stellar populations. However, the relation for
ETGs is linear and the one for the youngest galaxies is constant. We confirm
and improve the relation between average logarithmic total density slopes
$\overline{\gamma_{\rm T}}$ and $\sigma_{\rm e}$: $\overline{\gamma_{\rm T}}$
become steeper with increasing $\sigma_{\rm e}$ until $\lg(\sigma_{\rm e}/{\rm
km\,s^{-1}})\approx 2.2$ and then remain constant around $\overline{\gamma_{\rm
T}}\approx -2.2$. The $\overline{\gamma_{\rm T}}-\sigma_{\rm e}$ variation is
larger for LTGs than ETGs. At fixed $\sigma_{\rm e}$ the total density profiles
steepen with galaxy age and for ETGs. We find generally low dark matter
fractions, median $f_{\rm DM}(<R_{\rm e})=8$ per cent, within a sphere of
radius $R_{\rm e}$. However, we find that $f_{\rm DM}(<R_{\rm e})$ depends on
$\sigma_{\rm e}$ better than stellar mass: dark matter increases to a median
$f_{\rm DM}(<R_{\rm e})=33$ percent for galaxies with $\sigma_{\rm
e}\lesssim100{\rm km\,s^{-1}}$. The increased $f_{\rm DM}(<R_{\rm e})$ at low
$\sigma_{\rm e}$ explains the parabolic $\lg(M/L)_{\rm e}-\lg\sigma_{\rm e}$
relation.
