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In this paper, an investigation on the relative importance of the thermalgas, radiation, and (minimum-energy) magnetic pressures around $\approx$200star-forming regions in a sample of nearby normal and luminous infraredgalaxies is presented. Given the range of galaxy distances, pressure estimatesare made on spatial scales spanning $\sim$0.1$-3$kpc. The ratio of thermalgas-to-radiation pressures does not appear to significantly depend on starformation rate surface density ($\Sigma_{\rm SFR}$), but exhibits a steadydecrease with increasing physical size of the aperture over which thequantities are measured. The ratio of magnetic-to-radiation pressures appearsto be relatively flat as a function of $\Sigma_{\rm SFR}$ and similar in valuefor both nuclear and extranuclear regions, but unlike the ratio of thermalgas-to-radiation pressures, exhibits a steady increase with increasing aperturesize. Furthermore, it seems that the magnetic pressure is typically weaker thanthe radiation pressure on sub-kpc scales, and only starts to play a significantrole on few-kpc scales. When the internal pressure terms are summed, theirratio to the ($\Sigma_{\rm SFR}$-inferred) kpc-scale dynamical equilibriumpressure estimates is roughly constant. Consequently, it appears that thephysical area of the galaxy disk, and not necessarily environment (e.g.,nuclear vs. extranuclear regions) or star formation activity, may play thedominant role in determining which pressure term is most active aroundstar-forming regions. These results are consistent with a scenario in which acombination of processes acting primarily on different physical scales workcollectively to regulate the star formation process in galaxy disks.

The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures Around Star-Forming Regions in Normal Galaxies and Dusty Starbursts