  We study the spatial clustering through the projected two-point correlation
function of $632$ $(1130)$ XMM-COSMOS Active Galactic Nuclei (AGNs) with known
spectroscopic (spectroscopic or photometric) redshifts in the range $z = [0.1 -
2.5]$ in order to measure the AGN bias and estimate the typical mass of the
hosting dark matter (DM) halo as a function of AGN host galaxy properties. We
create AGN subsamples in terms of stellar mass $M_*$ and specific black hole
accretion rate $L_X/M_*$, to probe how AGN environment depends on these
quantities. For the full spectroscopic AGN sample, we measure a typical DM halo
mass of $\log (M_\mathrm{halo} / h^{-1}\mathrm{M}_\odot)=
12.79_{-0.43}^{+0.26}$, similar to galaxy group environments and in line with
previous studies for moderate-luminosity X-ray selected AGN. We find no
significant dependence on $L_X/M_*$, with $\log (M_\mathrm{halo} /
h^{-1}\mathrm{M}_\odot) = 13.06_{-0.38}^{+0.23}$ ($12.97_{-1.26}^{+0.39}$) for
the low (high) $L_X/M_*$ subsample. We also find no difference in the hosting
halos in terms of $M_*$ with $\log (M_\mathrm{halo} / h^{-1}\mathrm{M}_\odot) =
12.93_{-0.62}^{+0.31}$ ($12.90_{-0.62}^{+0.30}$) for the low (high) $M_*$
subsample. By comparing the $M_*-M_\mathrm{halo}$ relation derived for
XMM-COSMOS AGN subsamples with what is expected for normal non-active galaxies
by abundance matching and clustering results, we find that the typical DM halo
mass of our high $M_*$ AGN subsample is similar to that of non-active galaxies.
However, AGNs in our low $M_*$ subsample are found in more massive halos than
non-active galaxies. By excluding AGNs in galaxy groups from the clustering
analysis, we find evidence that the result for low $M_*$ may be due a larger
fraction of AGNs as satellites in massive halos.
