in (\[unu\]) with the standard parametric form of mixing matrix given in (\[PMNS\]), the neutrino mixing angles can be evaluated as [@Karmakar:2014dva] $$\begin{aligned}
 \sin^2\theta_{13}&=&\frac{2}{3}|\sin\theta|^2\\
 \sin^2\theta_{12}&=&\frac{1}{3(1- \sin^2\theta_{13})}\\
 \sin^2\theta_{23}&=&\frac{1}{2}+\frac{1}{\sqrt{2}}\sin\theta_{13}\sin\psi. \end{aligned}$$ Thus, the neutrino mixing angles are function of the angle $\theta$ which depends upon $x_{1,2}$ and they further depend upon the coupling constants $y_{1,2,3}$ as described before. Now, the neutrino mass eigenvalues can be written as $$\begin{aligned}
 m_{1}&=&v^2x_3/|a|\sqrt{1+\alpha^2+2\alpha\cos\phi_{ba}}\label{m1}\\
m_{2}&=&v^2x_4/|a| \label{m2}\\
m_{3}&=&v^2x_3/|a|\sqrt{1+\alpha^2-2\alpha\cos\phi_{ba}}\label{m3}, \end{aligned}$$ where $\alpha=|b|/|a|$ and $\phi_{ba}=\phi_{b}-\phi_{a}$ is the phase difference between $b$ and $a$. Using these, one can now define a ratio of solar to atmospheric mass-squared differences ($\Delta{m}_{\odot}^{2}=\Delta{m_{21}^{2}}={m_{2}^{2}-m_{1}^{2}}$ and $|\Delta{m}_{A}^{2}|=|\Delta{m}^2_{31}|={m_{3}^{2}-m_{1}^{2}}
\approx|\Delta{m}^2_{32}|={m_{3}^{2}-m_{2}^{2}}$ respectively) defined by $$\begin{aligned}
\label{r}
 r=\frac{\Delta{m}_{\odot}^{2}}{|\Delta{m}_{A}^{2}|}
 =\frac{(x_4^2(\alpha^2+2\alpha\cos\phi_{ba})-x_3^2)(1+\alpha^2-2\alpha\cos\phi_{ba})}{\pm x_3^24\alpha\cos\phi_{ba}}. \end{aligned}$$ Here, depending on the sign of denominator, the parameter space is divided into two parts: ’+’ in the denominator yields normal hierarchy of neutrino mass whereas for ’-’ in the denominator yields inverted neutrino mass hierarchy. Therefore, the neutrino mixing angles and the ratio of solar to atmospheric mass-squared differences are altogether functions of five parameters, namely three coupling constants $y_1,y_2,y_{3}$ and $\alpha,\phi_{ba}$. Using the observed neutrino oscillation data summarised in latest global fit [@Esteban:2018azc], these parameters can be constrained for both normal and inverted neutrino mass hierarchy, as we discuss 