energy as $${ V(\braket{ \Phi}) \simeq}
{ -3 e^{K_{N}}|W_{N}\left[\braket{ \Phi}\right]|^{2} \simeq}
{ -3\left(\frac{4}{5}\right)^{2}}{ v}^{ 4}\left(\frac{{ v}^{2}}{{ g}}\right)^{1/2}.$$ We assume that the negative vacuum energy is cancelled out by a supersymmetry-breaking effect which gives a positive contribution ${ \Lambda}_{\mathrm{SUSY}}^{4}$ to the vacuum energy. Thus, we have a relation between $ v$ and the gravitino mass $ m_{3/2}$ as $${ m_{3/2} \simeq}
{ \frac{{ \Lambda}_{\mathrm{SUSY}}^{2}}{\sqrt{3}}=}
{\frac{4}{5}}{ v}^{ 2}\left(\frac{{ v}^{ 2}}{ g}\right)^{ 1/4}.$$ To discuss the dynamics of the new inflation, we identify the inflaton field $\phi$ with the real part of the field $\Phi$ as $\phi \equiv \sqrt{2}Re{ \Phi}$. Neglecting the higher-order terms, we obtain the scalar potential of the new inflation as $${ V_{H}\left[ \phi\right] \simeq}
{ v}^{4} -{ \frac{C_{N}}{2}}{ v}^{ 4}{ \phi}^{ 2}
-\frac{ g}{ 2}{ v}^{ 2}{ \phi}^{ 4}
+\frac{{ g}^{ 2}}{ 16}{ \phi}^{ 8}.$$ We differentiate the scalar potential as $${\frac{dV_{N}}{d{\phi}} = }
{ -C_{N}}{ v}^{ 2}{ \phi} 
{ -2}{ g}{ v}^{ 2}{ \phi}^{ 3}
+\frac{{ g}^{2}}{ 2}{ \phi}^{ 7}.$$ When ${\phi}$ is smaller than ${\phi}_{d}\equiv\sqrt{C_Nv^2/(2g)}$, the first term dominantly controls the inflation dynamics. On the other hand, when $ \phi$ is larger than ${ \phi}_{d}$, the second term dominantly controls the inflation dynamics. New inflation occurs when 