  We present the results of a multi-frequency, time-averaged analysis of
blazars included in the Candidate Gamma-ray Blazar Survey catalog. Our sample
consists of 324 $\gamma$-ray detected ($\gamma$-ray loud) and 191 non
$\gamma$-ray detected ($\gamma$-ray quiet) blazars, and we consider all the
data up to 2016 April 1. We find that both the $\gamma$-ray loud and the
$\gamma$-ray quiet blazar populations occupy similar regions in the WISE
color-color diagram, and in the radio and X-ray bands $\gamma$-ray loud sources
are brighter. A simple one-zone synchrotron inverse-Compton emission model is
applied to derive the physical properties of both populations. We find that the
central black hole mass and the accretion disk luminosity ($L_{\rm disk}$)
computed from the modeling of the optical-UV emission with a Shakura-Sunyaev
disk reasonably matches with that estimated from the optical spectroscopic
emission-line information. A significantly larger Doppler boosting in the
$\gamma$-ray loud blazars is noted, and their jets are more radiatively
efficient. On the other hand, the $\gamma$-ray quiet objects are more
MeV-peaked, thus could be potential targets for next-generation MeV missions.
Our results confirm the earlier findings about the accretion-jet connection in
blazars; however, many of the $\gamma$-ray quiet blazars tend to deviate from
the recent claim that the jet power exceeds $L_{\rm disk}$ in blazars. A
broadband study, considering a larger set of $\gamma$-ray quiet objects and
also including BL Lacs, will be needed to confirm/reject this hypothesis and
also to verify the evolution of the powerful high-redshift blazars into their
low-power nearby counterparts.
