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The HII regions are all studied employing the same general prescriptions,despite the possible influence of their environment in their star formationprocesses. Through the analysis of two samples of 725 inner and 671 outer diskHII region observed spectra, we explore possible systematic differences betweentheir ionising clusters physical properties (metallicity, mass, and age),comparing observations and predictions by photoionisation models. Highermetallicities are confirmed for inner regions, although there are importantdiscrepancies between the diagnostic diagrams. Calibrations based on the N2index may underestimate inner regions O/H due to the [NII] saturation at solarmetallicities. The degeneracy between the age and ionisation parameter affectsO/H calibrations based on the O3N2 index. Innermost regions have enhanced N/Oratios, indicating an increase in the slope of the relation between N/O andO/H. Ionisation parameter calibrations based on the [SII]/H{\alpha} ratio arenot valid for inner regions due to the bivalued behaviour of this ratio withO/H. Innermost regions have lower [OII]/[OIII] ratios than expected, indicatinga possible non-linear relation between u and Z. Ionising and non-ionisingpopulations are present in both inner and outer regions. Inner regions showlarger ionising cluster masses that possibly compose star-forming complexes.Outer regions might be affected by stochastic effects. Equivalent widthsindicate younger ages for outer regions, but degeneracy between evolution andunderlying population effects prevent a quantitative determination. Innerregions have larger angular sizes, lower filling factors, and larger ionisedhydrogen masses. The confirmed systematic differences between ionising clustersof inner and outer HII regions condition the validity and range of reliabilityof O/H and u calibrations commonly applied to the study of HII regions.

Inner and outer star forming regions over the disks of spiral galaxies. II. A comparative of physical properties and evolutionary stages