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We explore the connection between different classes of active galactic nuclei(AGNs) and the evolution of their host galaxies, by deriving host galaxyproperties, clustering, and Eddington ratios of AGNs selected in the radio,X-ray, and infrared. We study a sample of 585 AGNs at 0.25 < z < 0.8 usingredshifts from the AGN and Galaxy Evolution Survey (AGES) and data in the radio(WSRT 1.4 GHz), X-rays (Chandra XBootes), and mid-IR (IRAC Shallow Survey). Theradio, X-ray, and IR AGN samples show modest overlap, indicating that to theflux limits of the survey, they represent largely distinct classes of AGNs. Wederive host galaxy colors and luminosities, as well as Eddington ratios(lambda), for obscured or optically faint AGNs. We also measure the two-pointcross-correlation between AGNs and galaxies on scales of 0.3-10 h^-1 Mpc, andderive typical dark matter halo masses. We find that: (1) radio AGNs are mainlyfound in luminous red galaxies, are strongly clustered (with M_halo ~ 3x10^13h^-1 M_sun), and have very low lambda <~ 10^-3; (2) X-ray-selected AGNs arepreferentially found in galaxies in the "green valley" of color-magnitude spaceand are clustered similarly to typical AGES galaxies (M_halo ~ 10^13 h^-1M_sun), with 10^-3 <~ lambda <~ 1; (3) IR AGNs reside in slightly bluer, lessluminous galaxies than X-ray AGNs, are weakly clustered (M_halo <~ 10^12 h^-1M_sun), and have lambda > 10^-2. We interpret these results in terms of asimple model of AGN and galaxy evolution, whereby a "quasar" phase and thegrowth of the stellar bulge occurs when a galaxy's dark matter halo reaches acritical mass between ~10^12 and 10^13 M_sun. Subsequently, star formationceases and AGN accretion shifts from radiatively efficient (optical- and IR-bright) to radiatively inefficient (optically-faint, radio-bright) modes.

Host galaxies, clustering, Eddington ratios, and evolution of radio, X-ray, and infrared-selected AGNs