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The relationships between atomic and molecular hydrogen and dust of varioussizes in extragalactic star-forming regions are considered, based onobservational data from the Spitzer and Herschel infrared space telescopes, theVery Large Array (atomic hydrogen emission) and IRAM (CO emission). The sourcesample consists of approximately 300 star-forming regions in 11 nearbygalaxies. Aperture photometry has been applied to measure the fluxes in eightinfrared bands (3.6, 4.5, 5.8, 8, 24, 70, 100, and 160$\mu$m), the atomichydrogen (21cm) line and CO (2--1) lines.  The parameters of the dust in the starforming regions were determined viasynthetic-spectra fitting, such as the total dust mass, the fraction ofpolycyclic aromatic hydrocarbons (PAHs), etc. Comparison of the observed fluxeswith the measured parameters shows that the relationships between atomichydrogen, molecular hydrogen, and dust are different in low- andhigh-metallicity regions. Low-metallicity regions contain more atomic gas, butless molecular gas and dust, including PAHs. The mass of dust constitutes about$1\%$ of the mass of molecular gas in all regions considered. Fluxes producedby atomic and molecular gas do not correlate with the parameters of the stellarradiation, whereas the dust fluxes grow with increasing mean intensity ofstellar radiation and the fraction of enhanced stellar radiation. The ratio ofthe fluxes at 8 and 24$\mu$m, which characterizes the PAH content, decreaseswith increasing intensity of the stellar radiation, possibly indicatingevolutionary variations of the PAH content. The results confirm that thecontribution of the 24$\mu$m emission to the total IR luminosity ofextragalactic star-forming regions does not depend on the metallicity.

Relation between parameters of dust and parameters of molecular and atomic gas in extragalactic star-forming regions