  We report JVLA 8-10 GHz ($\lambda$=3.0-3.7 cm) monitoring observations toward
the YSO cluster R Coronae Australis (R\,CrA), taken in 2012, from March 15 to
September 12. These observations were planned to measure the radio flux
variabilities in timescales from 0.5 hours to several days, to tens of days,
and up to $\sim$200 days. We found that among the YSOs detectable in individual
epochs, in general, the most reddened objects in the \textit{Spitzer}
observations show the highest mean 3.5 cm Stokes \textit{I} emission, and the
lowest fractional variabilities on $<$200-day timescales. The brightest radio
flux emitters in our observations are the two reddest sources IRS7W and IRS7E.
In addition, by comparing with observations taken in 1996-1998 and 2005, we
found that the radio fluxes of these two sources have increased by a factor
$\sim$1.5. The mean 3.5-cm fluxes of the three Class I/II sources IRSI, IRS2,
and IRS6 appear to be correlated with their accretion rates derived by a
previous near infrared line survey. The weakly accreting Class I/II YSOs, or
those in later evolutionary stages, present radio flux variability on
$<$0.5-hour timescales. Some YSOs were detected only during occasional flaring
events. The source R\,CrA went below our detection limit during a few fading
events.
