  In this work, we present a spectral and temporal analysis of {\it Swift}/XRT
and {\it NuSTAR} observations of GRS 1716--249 during its recent 2016--2017
outburst. This low mass X-ray binary underwent an extraordinary outburst after
a long quiescence of 23 years, since its last major outburst in 1993. The
source was observed over two different epochs during 2017 April, 07 and 10. The
best fit joint spectral fitting in the energy range 0.5 $-$ 79.0 keV indicates
that the spectrum is best described by relatively cold, weak disk blackbody
emission, dominant thermal Comptonization emission, and a relativistically
broadened fluorescent iron K$\alpha$ emission line. We observed a clear
indication of a Compton hump around 30 keV. We also detected an excess feature
of $\sim1.3$ keV. Assuming a lamp-post geometry of the corona, we constrained
the inner disk radius for both observations to 11.92$^{+8.62}_{-11.92}$
R$_{ISCO}$ (i.e., an upper limit) and 10.39$^{+9.51}_{-3.02}$ R$_{ISCO}$ (where
R$_{ISCO}\equiv$ radius of the innermost stable circular orbit) for the first
epoch (E1) and second epoch (E2), respectively. A significant ($\sim5\sigma$)
type$-$C quasi-periodic oscillation (QPO) at $1.20\pm0.04$ Hz is detected for
the first time for GRS 1716--249, which drifts to $1.55\pm0.04$ Hz
($\sim6\sigma$) at the end of the second observation. The derived spectral and
temporal properties show a positive correlation between the QPO frequency and
the photon index.
