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In this work we analyze the spectroscopic properties of a large number of Hii regions, \sim2600, located in 38 galaxies. The sample of galaxies has beenassembled from the face-on spirals in the PINGS survey and a sample describedin M\'armol-Queralt\'o (2011, henceforth Paper I). All the galaxies wereobserved using Integral Field Spectroscopy with a similar setup, covering theiroptical extension up to \sim2.4 effective radii within a wavelength range from\sim3700 to \sim6900{\AA}. We develop a new automatic procedure to detect H iiregions, based on the contrast of the H{\alpha} intensity maps. Once detected,the procedure provides us with the integrated spectra of each individualsegmented region. A well-tested automatic decoupling procedure has been appliedto remove the underlying stellar population, deriving the main proper- ties ofthe strongest emission lines in the considered wavelength range (covering from[O ii] {\lambda}3727 to [S ii] {\lambda}6731). A final catalogue of thespectroscopic properties of these regions has been created for each galaxy. Inthe current study we focused on the understanding of the average properties ofthe H ii regions and their radial distributions. We find that the gas-phaseoxygen abundance and the H{\alpha} equivalent width present negative andpositive gradient, respectively. The distribution of slopes is statisticallycompatible with a random Gaussian distribution around the mean value, if theradial distances are measured in units of the respective effective radius. Nodifference in the slope is found for galaxies of different morphologies:barred/non-barred, grand-design/flocculent. Therefore, the effective radius isa universal scale length for gradients in the evolution of galaxies. Otherproperties have a larger variance across each object.

Integral field spectroscopy of a sample of nearby galaxies: II. Properties of the H ii regions