  This is the fifth paper in a series of investigations of the clustering
properties of luminous, broad-emission-line active galactic nuclei (AGN)
identified in the ROSAT All-Sky Survey (RASS) and Sloan Digital Sky Survey
(SDSS). In this work we measure the cross-correlation function (CCF) between
RASS/SDSS DR14 AGN with the SDSS CMASS galaxy sample at $0.44<z<0.64$. We apply
halo occupation distribution (HOD) modeling to the CCF along with the
autocorrelation function of the CMASS galaxies. We find that X-ray and
optically selected AGN at $0.44<z<0.64$ reside in statistically identical halos
with a typical dark matter halo mass of $M_{\rm DMH}^{\rm typ,AGN} \sim
10^{12.7}\,h^{-1}\,\rm{M}_\odot$. The acceptable HOD parameter space for these
two broad-line AGN samples have only statistically marginal differences caused
by small deviations of the CCFs in the one-halo-dominated regime on small
scales. In contrast to optically selected AGN, the X-ray AGN sample may contain
a larger population of satellites at $M_{\rm DMH} \sim
10^{13}\,h^{-1}\,\rm{M}_\odot$. We compare our measurements in this work with
our earlier studies at lower independent redshift ranges, spanning a look-back
time of 6 Gyr. The comparison over this wider redshift range of $0.07<z<0.64$
reveals: (i) no significant difference between the typical DMH masses of X-ray
and optically selected AGN, (ii) weak positive clustering dependencies of
$M_{\rm DMH}^{\rm typ,AGN}$ with $L_{\rm X}$ and $M_{\rm BH}$, (iii) no
significant dependence of $M_{\rm DMH}^{\rm typ,AGN}$ on Eddington ratio, and
(iv) the same DMH masses host more-massive accreting black holes at high
redshift than at low redshifts.
