  The first JWST observations of nearby galaxies have unveiled a rich
population of bubbles that trace the stellar feedback mechanisms responsible
for their creation. Studying these bubbles therefore allows us to chart the
interaction between stellar feedback and the interstellar medium, and the
larger galactic flows needed to regulate star formation processes globally. We
present the first catalog of bubbles in NGC628, visually identified using MIRI
F770W PHANGS-JWST observations, and use them to statistically evaluate bubble
characteristics. We classify 1694 structures as bubbles with radii between
6-552 pc. Of these, 31% contain at least one smaller bubble at their edge,
indicating that previous generations of star formation have a local impact on
where new stars form. On large scales, most bubbles lie near a spiral arm, and
their radii increase downstream compared to upstream. Furthermore, bubbles are
elongated in a similar direction to the spiral arm ridge-line. These azimuthal
trends demonstrate that star formation is intimately connected to the spiral
arm passage. Finally, the bubble size distribution follows a power-law of index
$p=-2.2\pm0.1$, which is slightly shallower than the theoretical value by
1-3.5$\sigma$ that did not include bubble mergers. The fraction of bubbles
identified within the shells of larger bubbles suggests that bubble merging is
a common process. Our analysis therefore allows us to quantify the number of
star-forming regions that are influenced by an earlier generation, and the role
feedback processes have in setting the global star formation rate. With the
full PHANGS-JWST sample, we can do this for more galaxies.
