The paper presents a new class of parametric interior solutions of Einstein–Maxwell field equations in general relativity for a static spherically symmetric distribution of a charged perfect fluid with a particular form of electric field intensity. This solution gives us wide range of parameter, K (0.69≤K≤7.1), for which the solution is well behaved hence, suitable for modeling of superdense star. For this solution the gravitational mass of a superdense object is maximized with all degree of suitability by assuming the surface density of the star equal to the normal nuclear density ρnm = 2.5×10^17 kg m^(-3). By this model we obtain the mass of the Crab pulsar M_Crab=1.401M_⊙ and the radius, R_Crab= 12.98 km constraining the moment of inertia I_(NS,45)>1.61 for the conservative estimate of Crab nebula mass 2M⨀ and M_Crab=2.0156M_⊙ with radius, R_Crab= 14.07 km constraining the moment of inertia I_(NS,45)>3.04 for the newest estimate of Crab nebula mass 4.6M⨀ which are quite well in agreement with the possible values of mass and radius of Crab pulsar. Besides this, our model yields the moments of inertia for PSR J0737-3039A and PSR J0737-3039B are I_A=1.4624×10^45 g cm^2 and I_B=1.2689×10^45 g cm^2 respectively. It has been observed that under well behaved conditions this class of parametric solution gives us the maximum gravitational mass of causal superdense object 2.8020M_⨀ with radius 14.49 km, surface redshift 0.4319, charge Q = 4.67×10^20C, and central density ρ_c=2.68ρ_nm.