Аннотация:We studied 102 star forming regions in seven spiral galaxies (NGC 628, NGC 783, NGC 2336, NGC 6217, NGC 6946, NGC 7331, and NGC 7678) on the basis of complex spectroscopic, photometric (UBVRI) and spectrophotometric (Halpha line) observations. Using data on the chemical composition and absorption in HII regions, obtained from spectroscopic observations, and using evolutionary models, we estimated physical parameters (ages and masses) of young stellar groupings embedded in HII regions. We found that the gas extinction, A(gas), which was determined from the Balmer decrement, does not correspond in some cases to the absorption A(stars) in the young stellar associations (complexes). This is due to the spatial oset relative Hii cloud of the stellar group related to it. It has been found that the condition A(gas) = A(stars) is not satised for the star forming regions, in which: 1) the contribution to the total emission of gas in the B and/or V bands is higher than 40%, and 2) EW(Halpha) > 1500A. Extinction A(V) in studied star forming regions corrected for the Galactic absorption A(V)Gal ranges from 0 to 3 mag with a mean value A(V)-A(V)Gal = 1.18+-0.84 mag. We estimated masses and ages for 63 star forming regions. The regions have ages ranging from 1 to 10 Myr, the most part of them are younger than 6 Myr. The derived masses of young stellar groupings range from 10^4 Msun in the nearby galaxies NGC 628 and NGC 6946 to 10^7 Msun in the most distant NGC 7678. More than 80% of groupings have masses between 10^5 Msun and 10^6 Msun. The lowest mass estimate of ~1*10^4 Msun for the objects in NGC 628 and NGC 6946 belongs to the mass interval of the youngest Galactic open clusters.