We use high-resolution {sl Hubble Space Telescope} imaging observations of the young ($sim 15-25$ Myr-old) star cluster NGC 1818 in the Large Magellanic Cloud to derive an estimate for the binary fraction of F stars ($1.3 < M_star/M_odot < 1.6$). Thi
s study provides the strongest constraints yet on the binary fraction in a young star cluster in a low-metallicity environment (${[Fe/H]} sim -0.4$ dex). Employing artificial-star tests, we develop a simple method that can efficiently measure the probabilities of stellar blends and superpositions from the observed stellar catalog. We create synthetic color-magnitude diagrams matching the fundamental parameters of NGC 1818, with different binary fractions and mass-ratio distributions. We find that this method is sensitive to binaries with mass ratios, $q ga 0.4$. For binaries with F-star primaries and mass ratios $q > 0.4$, the binary fraction is $sim 0.35$. This suggests a total binary fraction for F stars of 0.55 to unity, depending on assumptions about the form of the mass-ratio distribution at low $q$.
