  We present low-frequency radio observations of the Galactic symbiotic
recurrent nova RS Ophiuchi during its 2021 outburst. The observations were
carried out with the upgraded Giant Metrewave Radio Telescope (uGMRT) spanning
a frequency range of 0.15$-$1.4 GHz during 23$-$287 days post the outburst. The
average value of the optically thin spectral index is $\alpha \sim$ $-$0.4
($F_{\nu} \propto \nu^\alpha$), indicating a non-thermal origin of the radio
emission at the observed frequencies. The radio light curves are best
represented by shock-driven synchrotron emission, initially absorbed by a
clumpy ionized circumbinary medium. We estimate the mass-loss rate of the red
giant companion star to be $\dot{M} \sim$ 7.5 $\times$ 10$^{-8}$ $M_{\odot}$
yr$^{-1}$ for an assumed stellar wind velocity of 20 km/s. The 0.15--1.4 GHz
radio light curves of the 2021 outburst are systematically brighter than those
of the 2006 outburst. Considering similar shock properties between the two
outbursts, this is indicative of a relatively higher particle number density in
the synchrotron emitting plasma in the current outburst.
