It is well known that fast CMEs are mostly associated with MHDshocks in the solar corona, leading to the formation of type II radio bursts.However, the absence of type II radio burst is not uncommon. Herein, we aim toanalyze the differences between the radio loud (RL) and radio quiet (RQ) fastCoronal Mass Ejections (CMEs) (speed ≥ 900 km s−1) during solar cycle 24(2008-2021). Among the selected 309 CMEs, we identified the associated flaresfor 143 events using running difference images from (i) Solar Dynamic Observatory/Atmospheric Imaging Assembly (SDO/AIA) observations and (ii) LargeAngle Spectrometric Coronagraph (LASCO). Among these 143 events, RQ andRL groups have 70 and 73 events, respectively. CALLISTO and Wind/WAVESobservations are used to identify these RL and RQ sets. We analyzed the possibilitiesof streamer-CME and CME-CME interaction. In this study, we reportthe important differences between RL and RQ CMEs and the underlying reasonsfor the radio quietness of fast CMEs. In the LASCO field of view, the majorityof RL CMEs (almost 90%) interacted with streamers and/or pre-CMEs, whereasonly 25% of RQ CMEs did the same, and there was no pre-CME interaction.The observational evidence led to the conclusion that substantial density perturbation/interaction increases the probability of production of type II radioemissions by shock of RL CMEs.