  We present the measurement of total and stellar/dark matter decomposed mass
density profile around a sample of galaxy groups and clusters with dynamical
masses derived from integral-field stellar kinematics from the MaNGA survey in
Paper I and weak lensing derived from the DECaLS imaging survey. Combining the
two data sets enables accurate measurement of the radial density distribution
from several kpc to Mpc scales. Intriguingly, we find that the excess surface
density derived from stellar kinematics in the inner region cannot be explained
by simply adding an NFW dark matter halo extrapolated from lensing measurement
at a larger scale to a stellar mass component derived from the NASA-Sloan Atlas
(NSA) catalogue. We find that a good fit to both data sets requires a stellar
mass normalization about 3 times higher than that derived from the NSA
catalogue, which would require an unrealistically too-heavy initial mass
function for stellar mass estimation. If we keep the stellar mass normalization
to that of the NSA catalogue but allow a varying inner dark matter density
profile, we obtain an asymptotic slope of $\gamma_{\rm gnfw}$=
$1.82_{-0.25}^{+0.15}$ and $\gamma_{\rm gnfw}$= $1.48_{-0.41}^{+0.20}$ for the
group bin and the cluster bin respectively, significantly steeper than the NFW
case. We also compare the total mass inner density slopes with those from
TNG300 and find that the values from the simulation are lower than the
observation by about $2\sigma$ level.
