We constrain the properties of massive binaries by comparing radial velocity data on early-type stars in Cygnus OB2 with the expectations of Monte Carlo models. Our comparisons test several popular prescriptions for massive binary parameters. We explore a range of true binary fraction, F, a range of power-law slopes, α, describing the distribution of companion masses between the limits q_(low) and 1, and a range of power-law slopes, β, describing the distribution of orbital separations between the limits r_(in) and r_(out). We also consider distributions of secondary masses described by a Miller-Scalo type IMF and by a two-component IMF that includes a substantial "twin" population with M_2 (approx =) M_1. Several seemingly disparate prescriptions for massive binary characteristics can be reconciled by adopting carefully chosen values for F, r_(in), and r_(out). We show that binary fractions F ＜ 0.7 are less probable than F ＞ 0.8 for reasonable choices of r_(in) and r_(out). Thus, the true binary fraction is high. For F = 1.0 and a distribution of orbital separations near the canonical "Opik's law distribution (i.e., flat; β = 0), the power-law slope of the mass ratio distribution is α = -0.6 to 0.0. For F (approx =) 0.8, α is somewhat larger, in the range -0.4 to 1.0. In any case, the secondary star mass function is inconsistent with a Miller-Scalo-like IMF unless the lower end is truncated below ～2-4 M_☉. In other words, massive stars preferentially have massive companions. The best-fitting models are described by a Salpeter or Miller-Scalo IMF for 60% of secondary star masses with the other ～40% of secondaries having M_2 (approx =) M_1, i.e., "twins." These model parameters simultaneously predict the fraction of Type Ib/c supernovae to be 30%-40% of all core-collapse supernovae, in agreement with recent observational estimates.
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