This paper investigates the evolution of dark energy (DE) at low redshift using data from the DESI Early Data Release, Pantheon+ Type Ia supernovae (SNeIa), and redshift space distortions (RSDs). The study employs a quadratic parametrization, $ X(z) $, to represent the DE density, allowing for the detection of DE evolution. The analysis includes the angular acoustic scale from the cosmic microwave background (CMB) to assess its impact on cosmological parameters. The results show evidence for DE evolution in all cases, both with and without the angular acoustic scale. The DE density begins to exhibit dynamical behavior at $ z \sim 0.5 $, assuming negative values beyond $ z \sim 1.5 $. The data show no significant preference for $ X(z) $ CDM over $ \Lambda $ CDM, with both models performing equally well according to the reduced $ \chi^2 $ and Durbin-Watson statistics. The study uses a quadratic parametrization for $ X(z) $, which is a second-degree polynomial that allows for a natural non-linear deviation from unity. This parametrization is used to reconstruct $ X(z) $ and analyze the evolution of DE. The results indicate that $ X(z) $ deviates from unity in all cases, suggesting DE evolution. The reconstructed $ X(z) $ shows that DE density starts to exhibit dynamical behavior at $ z \sim 0.5 $, with negative values beyond $ z \sim 1.5 $. The analysis also considers the effect of varying parameters such as $ N_{eff} $, $ \omega_b $, and $ z_d $ on the resulting cosmological parameters. The inclusion of CMB information in the form of the angular acoustic scale lowers $ H_0 $ in all analyses. The study finds that both $ X(z) $ CDM and $ \Lambda $ CDM models perform well in terms of goodness of fit, with no significant preference for one over the other. The results suggest that $ X(z) $ CDM does not resolve the Hubble tension, as it does not rectify the discrepancy between $ H_0 $ values from different datasets. However, the model may still offer insights into the nature of DE at low redshift, with the data preferring $ 0 < x_1 < 1 $ and $ x_2 < -1 $, indicating dynamical DE behavior. The study concludes that $ X(z) $ CDM is a viable model for exploring DE evolution at low redshift, although it does not resolve the Hubble tension.This paper investigates the evolution of dark energy (DE) at low redshift using data from the DESI Early Data Release, Pantheon+ Type Ia supernovae (SNeIa), and redshift space distortions (RSDs). The study employs a quadratic parametrization, $ X(z) $, to represent the DE density, allowing for the detection of DE evolution. The analysis includes the angular acoustic scale from the cosmic microwave background (CMB) to assess its impact on cosmological parameters. The results show evidence for DE evolution in all cases, both with and without the angular acoustic scale. The DE density begins to exhibit dynamical behavior at $ z \sim 0.5 $, assuming negative values beyond $ z \sim 1.5 $. The data show no significant preference for $ X(z) $ CDM over $ \Lambda $ CDM, with both models performing equally well according to the reduced $ \chi^2 $ and Durbin-Watson statistics. The study uses a quadratic parametrization for $ X(z) $, which is a second-degree polynomial that allows for a natural non-linear deviation from unity. This parametrization is used to reconstruct $ X(z) $ and analyze the evolution of DE. The results indicate that $ X(z) $ deviates from unity in all cases, suggesting DE evolution. The reconstructed $ X(z) $ shows that DE density starts to exhibit dynamical behavior at $ z \sim 0.5 $, with negative values beyond $ z \sim 1.5 $. The analysis also considers the effect of varying parameters such as $ N_{eff} $, $ \omega_b $, and $ z_d $ on the resulting cosmological parameters. The inclusion of CMB information in the form of the angular acoustic scale lowers $ H_0 $ in all analyses. The study finds that both $ X(z) $ CDM and $ \Lambda $ CDM models perform well in terms of goodness of fit, with no significant preference for one over the other. The results suggest that $ X(z) $ CDM does not resolve the Hubble tension, as it does not rectify the discrepancy between $ H_0 $ values from different datasets. However, the model may still offer insights into the nature of DE at low redshift, with the data preferring $ 0 < x_1 < 1 $ and $ x_2 < -1 $, indicating dynamical DE behavior. The study concludes that $ X(z) $ CDM is a viable model for exploring DE evolution at low redshift, although it does not resolve the Hubble tension.