Using spatially resolved H alpha emission line maps of star-forming galaxies, we study the spatial distribution of star formation over a wide range in redshift (0.5 less than or similar to z less than or similar to 1.7). Our z similar to 0.5 measurements come from deep Hubble Space Telescope (HST) Wide Field Camera 3 G102 grism spectroscopy obtained as part of the CANDELS Ly alpha Emission at Reionization Experiment. For star-forming galaxies with log(M (*)/M (circle dot)) >= 8.96, the mean H alpha effective radius is 1.2 +/- 0.1 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 similar to 1 and z similar to 1.7 from the 3D-HST and KMOS3D surveys, respectively, implying no redshift evolution. However, we observe redshift evolution in the stellar mass surface density within 1 kpc (sigma(1kpc)). Star-forming galaxies at z similar to 0.5 with a stellar mass of log(M (*)/M (circle dot)) = 9.5 have a ratio of sigma(1kpc) in H alpha relative to their stellar continuum that is lower by (19 +/- 2)% compared to z similar to 1 galaxies. sigma(1kpc,H alpha )/sigma(1kpc,Cont) decreases toward higher stellar masses. The majority of the redshift evolution in sigma(1kpc,H alpha )/sigma(1kpc,Cont) versus stellar mass stems from the fact that log(sigma(1kpc,H alpha )) declines twice as much as log(sigma(1kpc,Cont)) from z similar to 1 to 0.5 (at a fixed stellar mass of log(M (*)/M (circle dot)) = 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(1kpc,H alpha ) from z similar to 1 to z similar to 0.5.