The nature of dark energy can be investigated not only by equation of state but also through
clustering and sound speed. In this research, we examine clustering of some dynamical dark energy
models namely, power-law (PL), Chavelier-Polarski-Linder (CPL) and Feng-Shen-Li (FSL). We
will go beyond zero-order and Free parameter of models constraints by using current available
data including Planck DR2, Baryonic Acoustic Oscillation (BAO) and Supernovae type Ia (SNIa)
observation and Hubble space telescope (HST). We investigate that PL as early dark energy has
different behavior rather than semi-LCDM models such as rapid potential changes, higher matter
density contrast due to crossing LCDM equation of state and matter behavior at early universe.
We quantify the importance of uncoupled dark energy clustering, PL exhibits strong clustering
with δP L > 0 which can grow faster than δm and semi-LCDM models produce void of dark energy
with powerless amplitude around 10−12. In the linear regime, density contrast, growth rate index
f(σ8) and gravitational potential computed. Furthermore, temperature anisotropy and matter power
spectrum by modification of CAMB for dynamical models obtained and ISW effect. PL shows
more ISW effect, more value for matter power spectrum at large scale around k=0.01.Tension
between HST and CMB for H0 disappears for all models.