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 γ-ray detected γ-ray loudand 191γ-ray undetected γ-ray quietblazars; we consider all the data up to 2016 April 1. We find that both the( γ-ray loud) and (γ-ray quiet ) blazar populations occupy similar regions in the WISE color–color diagram, and γ-ray loud and sources are brighter in the radio and X-ray bands. 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 accretion disk luminosity(L_disk)computed from the modeling of the optical-UV emission with a Shakura –Sunyaev disk reasonably matches that estimated from the optical spectroscopic emission-line information. A signi ficantly larger Doppler boosting in the γ-ray loud and blazars is noted, and their jets are more radiatively ef ficient. On the other hand,the γ-ray quiet objects are more MeV-peaked and thus could be potential targets for next-generation MeV missions. Our results con fi rm earlier findings about the accretion-jet connection in blazars; however, many of the γ-ray quiet blazars tend to deviate from the recent claim that the jet power exceeds L_disk in blazars. A broadband study, considering a larger set of γ-ray quiet  objects and also including BL Lacs, will be needed to con firm/reject this hypothesis as well as to verify the evolution of the powerful high-redshift blazars into their low-power nearby counterparts