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

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... vironment depends on these quantities. For the full spectroscopic AGN sample, we measure a typical DM halo mass of log (M_halo / h^-1M_)= 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_halo / h^-1M_) = 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_halo / h^-1M_) = 12.93_-0.62^+0.31 (12.90_-0.62^+0.30) for the low (high) M_* subsample. By comparing the M_*-M_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.