  We determine radial- and age-abundance gradients of the Small Magellanic
Cloud (SMC) using spectra of 2,062 red giant branch (RGB) field stars observed
by SDSS-IV / APOGEE-2S. With coverage out to $\sim$9 kpc in the SMC, these data
taken with the high resolution ($R \sim 22,500$) APOGEE $H$-band spectrograph
afford the opportunity to measure extensive radial gradients for as many as 24
abundance ratios. The SMC is found to have an overall metallicity gradient of
$-$0.0546 $\pm$ 0.0043 dex/kpc. Ages are calculated for every star to explore
the evolution of the different abundance gradients. As a function of age, many
of the gradients show a feature 3.66--5.58 Gyr ago, which is especially
prominent in the [X/H] gradients. Initially many gradients flatten until about
$\sim$5.58 Gyr ago, but then steepen in more recent times. We previously
detected similar evolutionary patterns in the Large Magellanic Cloud (LMC)
which are attributed to a recent interaction between the LMC and SMC. It is
inferred that the feature in the SMC gradients was caused by the same
interaction. The age-[X/Fe] trends, which track average [X/Fe] over time, are
flat, demonstrating a slow enrichment history for the SMC. When comparing the
SMC gradients to the LMC and MW, normalized to disk scale length
($R_\text{d}$), the [X/Fe] and [X/Mg] gradients are similar, but there is a
dichotomy between the dwarfs and the Milky Way (MW) for the [X/H] gradients.
The median MW [X/H] gradient around $-$0.125 dex/$R_\text{d}$ whilst the Clouds
have gradients of about $-$0.075 dex/$R_\text{d}$.
