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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 inredshift ($0.5<z<1.7$). Our $z\sim0.5$ measurements come from deep Hubble SpaceTelescope WFC3 G102 grism spectroscopy obtained as part of the CANDELSLyman-alpha Emission at Reionization (CLEAR) Experiment. For star-forminggalaxies with Log$(M_{*}/\mathrm{M}_{\odot})\geqslant8.96$, the mean H-alphaeffective radius is $1.2\pm0.1$ times larger than that of the stellarcontinuum, implying inside-out growth via star formation. This measurementagrees within $1\sigma$ with those measured at $z\sim1$ and $z\sim1.7$ from the3D-HST and KMOS-3D surveys respectively, implying no redshift evolution.However, we observe redshift evolution in the stellar mass surface densitywithin 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 aratio of $\Sigma_\mathrm{1kpc}$ in H-alpha relative to their stellar continuumthat is lower by $(19\pm2)\%$ compared to $z\sim1$ galaxies.$\Sigma_{1\mathrm{kpc, H}\alpha}$/$\Sigma_{1\mathrm{kpc,Cont}}$ decreasestowards higher stellar masses. The majority of the redshift evolution in$\Sigma_{1\mathrm{kpc,H}\alpha}$/$\Sigma_{1\mathrm{kpc,Cont}}$ versus stellarmass stems from the fact that Log($\Sigma_{1\mathrm{kpc, H}\alpha}$) declinestwice as much as Log($\Sigma_{1\mathrm{kpc, Cont}}$) from $z\sim 1$ to 0.5 (ata fixed stellar mass of Log$(M_{*}/\mathrm{M}_{\odot})=9.5$). By comparing ourresults to the TNG50 cosmological magneto-hydrodynamical simulation, we ruleout dust as the driver of this evolution. Our results are consistent withinside-out quenching following in the wake of inside-out growth, the former ofwhich drives the significant drop in $\Sigma_{1\mathrm{kpc, H}\alpha}$ from$z\sim1$ to $z\sim0.5$.

CLEAR: The Evolution of Spatially Resolved Star Formation in Galaxies between $0.5\lesssim z \lesssim1.7$ using H$\alpha$ Emission Line Maps