We present present the first analyses of the radial velocity and BV light curves for the eclipsing binary system, V335 Set. This double-lined eclipsing binary has an eccentricity of 0.14. BV photometric light curves and double-lined radial velocities were solved simultaneously using an improved version of the Wilson-Devinney computer program. The masses and radii of the component stars were obtained as M(1) = 2.02 +/- 0.01 M(circle dot), M(2) = 1.84 +/- 0.02 M(circle dot), R(1) = 2.03 +/- 0.02 R(circle dot) and R(2) = 1.60 +/- 0.01 R(circle dot). We estimated the semi-amplitudes of the radial velocity curves of the primary and secondary components as K(1) = 106.31 +/- 0.88 km s(-1) and K(2) = 116.94 +/- 0.88 km s(-1), respectively. As determined by absolute visual magnitude and corrections for interstellar extinction, the distance of the system from earth was found to be d = 219 +/- 24 pc. The existence of apsidal motion is presented as means of eclipse time, and the apsidal motion rate was found to be (omega) over dot(obs) = 0.01302 +/- 0.02563 deg cycle(-1). The corresponding apsidal motion period was found to be U = 261 514 years. Using the absolute properties and apsidal motion parameters obtained from period analysis, we computed the observational and theoretical internal structure constants to be logk(2,obs) = -1.53 and logk(2,theo) = -2.44, respectively. We also present the evolutionary status of the component stars in an H-R diagram using solar metallicity and four helium content values. Both component stars are slightly evolved from the ZAMS. (C) 2011 Elsevier B.V. All rights reserved.