  We analyze rest-frame ultraviolet to optical spectra of three $z\simeq7.47$ -
$7.75$ galaxies whose Ly$\alpha$-emission lines were previously detected with
Keck/MOSFIRE observations, using the JWST/NIRSpec observations from the Cosmic
Evolution Early Release Science (CEERS) survey. From NIRSpec data, we confirm
the systemic redshifts of these Ly$\alpha$ emitters, and emission-line ratio
diagnostics indicate these galaxies were highly ionized and metal poor. We
investigate Ly$\alpha$ line properties, including the line flux, velocity
offset, and spatial extension. For the one galaxy where we have both NIRSpec
and MOSFIRE measurements, we find a significant offset in their flux
measurements ($\sim5\times$ greater in MOSFIRE) and a marginal difference in
the velocity shifts. The simplest interpretation is that the Ly$\alpha$
emission is extended and not entirely encompassed by the NIRSpec slit. The
cross-dispersion profiles in NIRSpec reveal that Ly$\alpha$ in one galaxy is
significantly more extended than the non-resonant emission lines. We also
compute the expected sizes of ionized bubbles that can be generated by the
Ly$\alpha$ sources, discussing viable scenarios for the creation of sizable
ionized bubbles ($>$1 physical Mpc). The source with the highest-ionization
condition is possibly capable of ionizing its own bubble, while the other two
do not appear to be capable of ionizing such a large region, requiring
additional sources of ionizing photons. Therefore, the fact that we detect
Ly$\alpha$ from these galaxies suggests diverse scenarios on escape of
Ly$\alpha$ during the epoch of reionization. High spectral resolution spectra
with JWST/NIRSpec will be extremely useful for constraining the physics of
patchy reionization.
