We present the results of deep study of the open star cluster NGC752 based on our analysis of the Gaia EDR3 data (A.G.A. Brown, et al., A&A, vol. 649, A1,2021). An angular radius of NGC752, its distance from the Sun and the age are estimated as ~ 0.5∘, ~ 450 pc and 1.3–1.5 Gyr (M.A. Agüeros, et al., ApJ, vol. 862, 33 (2018), respectively, based on its known members (M. Agarwal, et al., MNRAS, vol. 502, 2582, 2021; S. Bhattacharya, et al., MNRAS, vol. 505, 1607, 2021). The ASteCA package (G.I. Perren, R.A. Vázquez, and A.E. Piatti, A&A, vol. 576, A6, 2015) was used for automated analysis of the main parameters of the cluster for statistical verification of the physical cluster true allocation from random super densities of field stars. The set of functions included in the code applies astrometric and photometric data to obtain objective precise values for the given coordinates of the cluster center, radius, luminosity function and integral value of the color index, accurate estimations of metallicity, age, redness and distance to the cluster by the isochron selection method based on the generation of synthetic cluster on the base of theoretical isochrones and the selection of the maximum match using a genetic algorithm. 44 new members of the cluster were reliably detected with a membership probability in the range from 0.81 to 1 (302 stars in total), which supplement the number of known member stars (258) within NGC 752 (M. Agarwal, et al., MNRAS, vol. 502, 2582, 2021; S. Bhattacharya, et al., MNRAS, vol. 505, 1607, 2021). We considered the stellar density profile from the center, the diagram of proper motions of the stars of the cluster NGC752 with mean values 𝜇𝛼cos𝛿 = 9.790 mas / yr, 𝜇𝛿= -11.784 mas / yr; the comparative histogram of parallaxes of the identified probable cluster members and the field stars and the initial mass function (IMF) with cluster z(metallicity)= 0.00797± 0.00087, log(age)=9.352±0.030 , distance modulus (m-M)0=8.258±0.023.