  How stellar feedback from high-mass stars (e.g., H{\sc ii} regions)
influences the surrounding interstellar medium and regulates new star formation
is still unclear. To address this question, we observed the G9.62+0.19 complex
in 850 $\mu$m continuum with the JCMT/POL-2 polarimeter. An ordered magnetic
field has been discovered in its youngest clump, the G9.62 clump. The magnetic
field strength is determined to be $\sim$1 mG. Magnetic field plays a larger
role than turbulence in supporting the clump. However, the G9.62 clump is still
unstable against gravitational collapse even if thermal, turbulent, and
magnetic field support are taken into account all together. The magnetic field
segments in the outskirts of the G9.62 clump seem to point toward the clump
center, resembling a dragged-in morphology, indicating that the clump is likely
undergoing magnetically-regulated global collapse. However, The magnetic field
in its central region is aligned with the shells of the photodissociation
regions (PDRs) and is approximately parallel to the ionization (or shock)
front, indicating that the magnetic field therein is likely compressed by the
expanding H{\sc ii} regions that formed in the same complex.
