  In our earlier 2019 paper, we evaluated the reliability of Schwarzschild's
orbit-superposition dynamical modelling method in estimating the internal mass
distribution, intrinsic stellar shapes and orbit distributions of early-type
galaxies (ETGs) taken from the Illustris cosmological simulation. We now apply
the same techniques to galaxies taken from the integral-field survey Mapping
Nearby Galaxies with APO (MaNGA), using a sample of 149 ETGs in the mass range
of $10^{9.90}\sim10^{11.80} M_{\odot}$ and made up of 105 central and 44
satellite galaxies. We find that low-mass ETGs with $\log(M_*/M_{\odot})<11.1$
have an average dark matter fraction of $\sim0.2$ within one effective radius
$R_{\rm e}$, tend to be oblate-like, and are dominated by rotation about their
minor axis. High-mass ETGs with $\log(M_*/M_{\odot})>11.1$ have an average dark
matter fraction of $\sim0.4$ within one effective radius $R_{\rm e}$, tend to
be prolate-like, and are dominated by rotation about their major axis and by
centrophilic orbits. The changes of internal structures within one $R_{\rm e}$
are dominated by the total stellar mass of the individual galaxies. We find no
differences of internal structures between central and satellite ETGs for the
same stellar masses. However, for similar stellar mass and colour
distributions, we find that ETGs more prolate-like, or with more hot orbits,
tend to have higher close neighbour counts at $r_p\sim40$ kpc.
