  We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles
of $>$500 $M_\star>10^{10}~M_\odot$ galaxies in the redshift range $0.5<z<2.3$.
We compare the resulting rest-frame 1.5-2$\mu$m half-light radii
($R_{\rm{NIR}}$) with stellar half-mass radii (\rmass) derived with multi-color
light profiles from CANDELS HST imaging. In general agreement with previous
work, we find that $R_{\rm{NIR}}$ and \rmass~are up to 40\%~smaller than the
rest-frame optical half-light radius $R_{\rm{opt}}$. The agreement between
$R_{\rm{NIR}}$ and \rmass~is excellent, with negligible systematic offset
($<$0.03 dex) up to $z=2$ for quiescent galaxies and up to $z=1.5$ for
star-forming galaxies. We also deproject the profiles to estimate \rmassd, the
radius of a sphere containing 50\% of the stellar mass. We present the
$R-M_\star$ distribution of galaxies at $0.5<z<1.5$, comparing $R_{\rm{opt}}$,
\rmass~and \rmassd. The slope is significantly flatter for \rmass~and \rmassd~
compared to $R_{\rm{opt}}$, mostly due to downward shifts in size for massive
star-forming galaxies, while \rmass~and \rmassd~do not show markedly different
trends. Finally, we show rapid size evolution ($R\propto (1+z)^{-1.7\pm0.1}$)
for massive ($M_\star>10^{11}~M_\odot$) quiescent galaxies between $z=0.5$ and
$z=2.3$, again comparing $R_{\rm{opt}}$, \rmass~and \rmassd. We conclude that
the main tenets of the size evolution narrative established over the past 20
years, based on rest-frame optical light profile analysis, still hold in the
era of JWST/NIRCam observations in the rest-frame near-IR.
