Properties of photospheric bright points (BPs) near an active region have been studied in TiO lambda 7058 angstrom images observed by the New Vacuum Solar Telescope of the Yunnan Observatories. We developed a novel recognition method that was used to identify and track 2010 BPs. The observed evolving BPs are classified into isolated (individual) and non-isolated (where multiple BPs are observed to display splitting and merging behaviors) sets. About 35.1% of BPs are non-isolated. For both isolated and non-isolated BPs, the brightness varies from 0.8 to. 1.3 times the average background intensity and follows a Gaussian distribution. The lifetimes of BPs follow a lognormal distribution, with characteristic lifetimes of (267 +/- 140). s and (421 +/- 255). s, respectively. Their size also follows log-normal distribution, with an average size of about (2.15 +/- 0.74). x. 10(4) km(2) and (3.00 +/- 1.31). x 10(4) km(2) for area, and (163 +/- 27) km and (191 +/- 40) km for diameter, respectively. Our results indicate that regions with strong background magnetic field have higher BP number density and higher BP area coverage than regions with weak background field. Apparently, the brightness/size of BPs does not depend on the background field. Lifetimes in regions with strong background magnetic field are shorter than those in regions with weak background field, on average.