  We study the stellar and star formation (SF) properties of the host galaxies
of 58 X-ray selected AGN in the GOODS portion of the Chandra Deep Field South
(CDF-S) region at z~0.5-1.4. The AGN are selected such that their rest-frame UV
to near-IR SEDs are dominated by stellar emission, i.e., they show a prominent
1.6micron bump, thus minimizing the AGN emission 'contamination'. This AGN
population comprises approximately 50% of the X-ray selected AGN at these
redshifts. Using models of stellar and dust emission we model their SEDs to
derive stellar masses (M*) and total (UV+IR) star formation rates (SFR). AGN
reside in the most massive galaxies at the redshifts probed here. Their
characteristic stellar masses (M*~7.8x10^10 Msun and M*~1.2x10^11 Msun at
median z of 0.67 and 1.07, respectively) appear to be representative of the
X-ray selected AGN population at these redshifts, and are intermediate between
those of local type 2 AGN and high redshift (z~2) AGN. The inferred black hole
masses (MBH~ 2x10^8 Msun) of typical AGN are similar to those of optically
identified quasars at similar redshifts. Since the AGN in our sample are much
less luminous (L(2-10keV)<10^44 erg/s) than quasars, typical AGN have low
Eddington ratios (eta~0.01-0.001). This suggests that, at least at intermediate
z, the cosmic AGN 'downsizing' is due to both a decrease in the characteristic
stellar mass of typical host galaxies, and less efficient accretion. Finally
there is no strong evidence in AGN host galaxies for either highly suppressed
SF (expected if AGN played a role in quenching SF) or elevated SF when compared
to mass selected (i.e., IRAC-selected) galaxies of similar stellar masses and
redshifts. This may be explained by the fact that galaxies with M*~5x 10^10 -
5x10^11 Msun are still being assembled at the redshifts probed here.
