  We investigate the emergence phase of young star clusters in the nearby
spiral galaxy NGC 628. We use JWST NIRCam and MIRI observations to create
spatially resolved maps of the Pa$\alpha$-1.87 $\mu$m and Br$\alpha$-4.05
$\mu$m hydrogen recombination lines, as well as the 3.3 $\mu$m and 7.7 $\mu$m
emission from polycyclic aromatic hydrocarbons (PAHs). We extract 953 compact
HII regions and analyze the PAH emission and morphology at $\sim$10 pc scales
in the associated photo-dissociation regions (PDRs). While HII regions remain
compact, radial profiles help us to define three PAH morphological classes:
compact ($\sim$ 42%), extended ($\sim$ 34%) and open ($\sim$ 24%). The majority
of compact and extended PAH morphologies are associated with very young star
clusters ($<$5 Myr), while open PAH morphologies are mainly associated with
star clusters older than 3 Myr. We observe a general decrease in the 3.3 $\mu$m
and 7.7 $\mu$m PAH band emission as a function of cluster age, while their
ratio remains constant with age out to 10 Myr and morphological class. The
recovered PAH$_{3.3 \mu{\rm m}}$/PAH$_{7.7 \mu{\rm m}}$ ratio is lower than
values reported in the literature for reference models that consider neutral
and ionized PAH populations and analyses conducted at galactic scales. The 3.3
$\mu$m and 7.7 $\mu$m bands are typically associated to neutral and ionised
PAHs, respectively. While we expected neutral PAHs to be suppressed in
proximity of the ionizing source, the constant PAH$_{3.3 \mu{\rm m}}$/PAH$_{7.7
\mu{\rm m}}$ ratio would indicate that both families of molecules disrupt at
similar rates in proximity of the HII regions.
