  We present spatially resolved, simple stellar population equivalent ages,
stellar metallicities, and abundance ratios for 456 massive
($10.3\lesssim\log(\mathrm{M}_*/\mathrm{M}_\odot)\lesssim11.8$) quiescent
galaxies at $0.6\lesssim z\lesssim1.0$ from the Large Early Galaxy Astrophysics
Census, derived using full-spectrum models. Typically, we find flat age and
[Mg/Fe] gradients, and negative [Fe/H] gradients, implying iron-rich cores. We
also estimate intrinsic [Fe/H] gradients via forward modelling. We examine the
observed gradients in three age bins. Younger quiescent galaxies typically have
negative [Fe/H] gradients and positive age gradients, possibly indicating a
recent central starburst. Additionally, this finding suggests that
photometrically measured flat colour gradients in young quiescent galaxies are
the result of the positive age and negative metallicity gradients cancelling
each other. For older quiescent galaxies, the age gradients become flat and
[Fe/H] gradients weaken, though remain negative. Thus, negative colour
gradients at older ages are likely driven by metallicity gradients. The
diminishing age gradient may result from the starburst fading. Furthermore, the
persistence of the [Fe/H] gradients may suggest that the outskirts are
simultaneously built up by mergers with lower metallicity satellites. On the
other hand, the gradients could be inherited from the star-forming phase, in
which case mergers may not be needed to explain our findings. This work
illustrates the need for resolved spectroscopy, instead of just photometry, to
measure stellar population gradients. Extending these measurements to higher
redshift is imperative for understanding how stellar populations in quiescent
galaxies are assembled over cosmic time.
