  The problem of the determination of T Tauri stars masses and ages using their
evolutionary status is discussed. We test of pre-main sequence evolutionary
models of D'Antona \& Mazzitelli (1994), Dotter et al. (2008), Bressan et al.
(2012) and Chen et al. (2014), Baraffe et al. (2015) using well determined
observational parameters of 12 binary T Tauri stars (TTS) and 2 binary red
dwarfs. It is shown that the masses derived using the tracks of all models are
in good agreement with the masses obtained from the observations of TTS with
masses $M > 0.7 M_{\odot}$ (mean error $\varepsilon\sim10\% $). Low-mass stars
with $M \le 0.7 M_{\odot}$ have significantly greater mean error: $\varepsilon
\sim 50\%$ for the tracks of Bressan et al. and Chen et al. and $\varepsilon
\sim 30\%$ for the other tracks. The isochrones of all tested evolutionary
models diverge for the stars with masses $M \le 0.7 M_{\odot}$. The difference
increases with the mass decrease and can reach 10\% of Kelvin-Helmholtz time
for stars with mass $M = 0.2 M_{\odot}$. The ages of most of the considered T
Tauri stars are smaller than the Kelvin-Helmholtz time. This confirms their
evolutionary status of pre-main sequence stars.
