The stellar content and environment of the Sh2-311 region have been studied using the deep optical and near-infrared (NIR) observations. The region contains three clusters, viz. NGC 2467, Haffner 18 and Haffner 19. NGC 2467 and Haffner 19 are found to be located in the Perseus arm at the distances of 5.0±0.4 kpc and 5.7±0.4 kpc, respectively whereas cluster Haffner 18 is located at the distance of 11.2±1.0 kpc. The NGC 2467 and Haffner 19 clusters might have been formed from the same molecular cloud, whereas the the cluster Haffner 18 is located in the outer galactic arm Norma-Cygnus. On the basis of deep NIR observations we have identified 73 young stellar sources (YSOs) with NIR-excess stars. The estimated ages and masses of these YSOs are in the range of 0.1-5.0 Myr and 0.3-3.5 M_sun, respectively suggesting that these sources could be T-Tauri stars. Spatial distribution of YSOs shows that some of the YSOs are distributed along the 8 µm emission contours derived from Spitzer IRAC observation, whereas a significant number of YSOs are clustered towards the eastern border of the 8 µm contours. The dynamical age of the ionized region, spatial distribution of YSOs, and mean age of the YSOs, (∼1.3 Myr) suggest for a triggered star formation in the Sh2-311 region probably due to the collect and collapse process. The IMF of the YSOs is found to be flat (Γ=0.08±0.22).