Abstract We present the results from a complex study of an eclipsing O-type binary (Aa+Ab) with the orbital period of P _A = 3.2254367 days that forms part of a higher-order multiple system in a configuration of (A+B)+C. We derived masses of the Aa+Ab binary of M ₁ = 19.02 ± 0.12 and M ₂ = 17.50 ± 0.13 M _⊙, the radii of R ₁ = 7.70 ± 0.05 and R ₂ = 6.64 ± 0.06 R _⊙, and temperatures of T ₁ = 34,250 ± 500 K and T ₂ = 33,750 ± 500 K. From the analysis of the radial velocities, we found a spectroscopic orbit of A in the outer A+B system with P _A+B = 195.8 days (P _A+B/P _A ≈ 61). In the O − C analysis, we confirmed this orbit and found another component orbiting the A+B system with P _AB+C = 2550 days (P _AB+C/P _A+B ≈ 13). From the total mass of the inner binary and its outer orbit, we estimated the mass of the third object, M _B ≳ 10.7 M _⊙. From the light travel time effect fit to the O − C data, we obtained the limit for the mass of the fourth component, M _C ≳ 7.3 M _⊙. These extra components contribute about 20%–30% (increasing with wavelength) to the total system light. From the comparison of model spectra with the multiband photometry, we derived a distance modulus of 18.59 ± 0.06 mag, a reddening of 0.16 ± 0.02 mag, and an R_V of 3.2. This work is part of our ongoing project, which aims to calibrate the surface brightness–color relation for early-type stars.