We present mid-infrared (MIR) spectra of H ii regions within star-forming galaxies M83 and M33. Their emission features are compared with Galactic and extragalactic H ii regions, H ii-type galaxies, starburst galaxies, and Seyfert/LINER type galaxies. Our main results are as follows: (i) the M33 and M83 H ii regions lie in between Seyfert/LINER galaxies and H ii-type galaxies in the 7.7/11.3 -6.2/11.3 plane, while the different sub-samples exhibiting different 7.7/6.2 ratios; (ii) Using the NASA Ames PAH IR Spectroscopic database, we demonstrate that the 6.2/7.7 ratio does not effectively track PAH size, but the 11.3/3.3 PAH ratio does; (iii) variations on the 17 µm PAH band depends on object type however, there is no dependence on metallicity for both extragalactic H ii regions and galaxies; (iv) the PAH/VSG intensity ratio decreases with the hardness of the radiation field and galactocentric radius (R g ), yet the ionization alone cannot account for the variation seen in all of our sources; (v) the relative strength of PAH features does not change significantly with increasing radiation hardness, as measured through the [Ne iii]/[Ne ii] ratio and the ionization index; (vi) We present PAH SFR calibrations based on the tight correlation between the 6.2, 7.7, and 11.3 µm PAH luminosities with the 24 µm luminosity and the combination of the 24 µm and Hα luminosity; (vii) Based on the total luminosity from PAH and FIR emission, we argue that extragalactic H ii regions are more suitable templates in modeling and interpreting the large scale properties of galaxies compared to Galactic H ii regions.

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