  We investigate spatially-resolved emission-line ratios in a sample of 219
galaxies ($0.6<z<1.3$) detected using the G102 grism on the \emph{Hubble Space
Telescope} Wide Field Camera 3, taken as part of the CANDELS Ly$\alpha$
Emission at Reionization (CLEAR) survey, to measure ionization profiles and
search for low-luminosity active galactic nuclei (AGN). We analyze \OIII\ and
\Hb\ emission-line maps, enabling us to spatially resolve the \OIIIHb\
emission-line ratio across the galaxies in the sample. We compare the \OIIIHb\
ratio in galaxy centers and outer annular regions to measure ionization
gradients and investigate the potential of sources with nuclear ionization to
host AGN. We investigate some of the individual galaxies that are candidates to
host strong nuclear ionization and find that they often have low stellar mass
and are undetected in X-rays, as expected for low-luminosity AGN in low-mass
galaxies. We do not find evidence for a significant population of off-nuclear
AGN or other clumps of off-nuclear ionization. We model the observed
distribution of \OIIIHb\ gradients and find that most galaxies are consistent
with small or zero gradients, but 6-16\% of galaxies in the sample are likely
to host nuclear \OIIIHb\ that is $\sim$0.5~dex higher than in their outer
regions. This study is limited by large uncertainties in most of the measured
\OIIIHb\ spatial profiles, therefore deeper data, e.g, from deeper
\textit{HST}/WFC3 programs or from \textit{JWST}/NIRISS, are needed to more
reliably measure the spatially resolved emission-line conditions of individual
high-redshift galaxies.
