  Using spatially resolved H-alpha emission line maps of star-forming galaxies,
we study the evolution of gradients in galaxy assembly over a wide range in
redshift ($0.5<z<1.7$). Our $z\sim0.5$ measurements come from deep Hubble Space
Telescope WFC3 G102 grism spectroscopy obtained as part of the CANDELS
Lyman-alpha Emission at Reionization (CLEAR) Experiment. For star-forming
galaxies with Log$(M_{*}/\mathrm{M}_{\odot})\geqslant8.96$, the mean H-alpha
effective radius is $1.2\pm0.1$ times larger than that of the stellar
continuum, implying inside-out growth via star formation. This measurement
agrees within $1\sigma$ with those measured at $z\sim1$ and $z\sim1.7$ from the
3D-HST and KMOS-3D surveys respectively, implying no redshift evolution.
However, we observe redshift evolution in the stellar mass surface density
within 1 kiloparsec ($\Sigma_\mathrm{1kpc}$). Star-forming galaxies at
$z\sim0.5$ with a stellar mass of Log$(M_{*}/\mathrm{M}_{\odot})=9.5$ have a
ratio of $\Sigma_\mathrm{1kpc}$ in H-alpha relative to their stellar continuum
that is lower by $(19\pm2)\%$ compared to $z\sim1$ galaxies.
$\Sigma_{1\mathrm{kpc, H}\alpha}$/$\Sigma_{1\mathrm{kpc,Cont}}$ decreases
towards higher stellar masses. The majority of the redshift evolution in
$\Sigma_{1\mathrm{kpc,H}\alpha}$/$\Sigma_{1\mathrm{kpc,Cont}}$ versus stellar
mass stems from the fact that Log($\Sigma_{1\mathrm{kpc, H}\alpha}$) declines
twice as much as Log($\Sigma_{1\mathrm{kpc, Cont}}$) from $z\sim 1$ to 0.5 (at
a fixed stellar mass of Log$(M_{*}/\mathrm{M}_{\odot})=9.5$). By comparing our
results to the TNG50 cosmological magneto-hydrodynamical simulation, we rule
out dust as the driver of this evolution. Our results are consistent with
inside-out quenching following in the wake of inside-out growth, the former of
which drives the significant drop in $\Sigma_{1\mathrm{kpc, H}\alpha}$ from
$z\sim1$ to $z\sim0.5$.
