We have determined Be abundances in 50 F and G dwarfs in the mass range of 0.9 ≤ M☉≤ 1.1 as determined by Lambert & Reddy. The effective temperatures are 5600-6400 K and metallicities from -0.65 to +0.11. The spectra were taken primarily with Keck I + HIRES. The Be abundances were found via spectral synthesis of Be II lines near 3130 Å. The Be abundances were investigated as a function of age, temperature, metallicity, and Li abundance in this narrow mass range. Even though our stars are similar in mass, they show a range in Be abundances of a factor of >40. We find that [Be/Fe] has no dependence on temperature, but does show a spread of a factor of 6 at a given temperature. The reality of the spread is shown by two identical stars that differ from each other by a factor of 2 only in their abundances of Li and Be. Our thin-disk star sample fits the trend between Be abundance and [Fe/H] found for halo and thick-disk stars, extending it to about 4 orders of magnitude in the two logarithmic quantities. Both Fe and Be appear to increase similarly over time in the Galaxy. One-third of our sample may be classified as subgiants; these more evolved stars have lower Be abundances than the dwarfs. They have undergone Be depletion by slow mixing on the main sequence and Be dilution during their trip toward the red giant base. There are both Li and Be detections in 60 field stars in the "Li-plateau" of 5900-6300 K now and the abundances of the two light elements are correlated with a slope of 0.34±0.05, with greater Li depletion than Be depletion.