The results of a combined near-infrared and IRAS mapping study of five H II regions are presented for which fairly complete information at optical and radio wavelengths previously existed. The near-infrared observations, carried out with the 2.1-m telescope at Observatorio de San Pedro Martir (Mexico), made it possible to study the stellar content at the core of each nebula, while an analysis of extended near-infrared emission zones showed these to arise mainly from ionized gas (S148 and S206) or through scattering and thermal emission from dust grains surrounding a massive young star (S269-IRS2). The analysis of IRAS data, on the other hand, suggests that two different populations of grains contribute to the observed 12- to 100-micron fluxes, and these are modeled with a small sized, PAH-type, grain component plus the 'standard' interstellar silicate grains.