  We report the discovery of intertwined/entangled sub-structures towards the
bubble wall of NGC 3324 below a physical scale of 4500 AU, which is the sharp
edge/ionization front/elongated structure traced at the interface between the
HII region and the molecular cloud. The sharp edge appears wavy in the Spitzer
3.6-8.0 $\mu$m images (resolution $\sim$2$''$). Star formation signatures have
mostly been traced on one side of the ionization front, which lies on the
molecular cloud's boundary. The James Webb Space Telescope's (JWST) near- and
mid-infrared images (resolution $\sim$0.07$''$-0.7$''$) are employed to resolve
the sharp edge, which has a curvature facing the exciting O-type stars. The
elongated structures are associated with the 3.3 $\mu$m polycyclic aromatic
hydrocarbon (PAH) emission, the 4.05 $\mu$m ionized emission, and the 4.693
$\mu$m H$_{2}$ emission. However, the PAH-emitting structures are depicted
between the other two. The H$_{2}$ emission reveals numerous intertwined
sub-structures which are not prominently traced in the 3.3 $\mu$m PAH emission.
The separation between two sub-structures in the H$_{2}$ emission is
$\sim$1.1$''$ or 2420 AU. The intertwined sub-structures are traced in the
spatial areas associated with the neutral to H$_{2}$ transition zone,
suggesting the origin of these structures by ``thin-shell'' instability.
Furthermore, an arc-like feature traced in the Spitzer 3.6-8.0 $\mu$m images is
investigated as a bipolar HII region (extent $\sim$0.35 pc) at T$_\mathrm{d}$
$\sim$25-28~K using the JWST images. A massive star candidate VPHAS-OB1 #03518
seems to be responsible for the bipolar HII region.
